| JAN_CONFIG_ALLON | No observations, but instrument ON for thermal stabilization of the complete electronics (PEU and detector are ON) and for setting the observation sequences and between two observation sequences that are too close to switch the detector OFF. | JANUS |
|---|
| PEL_JUPITER_IN_SITU_IMAGING_LOW_2 | Far approach from moon (flyby), setting up NIM filament | PEPLO |
|---|
| PEL_JUPITER_IN_SITU_IMAGING_BURST_2 | *Burst in-situ mode, magnetosphere
*CA of moon flybys with JNA/JENI imaging and high time (plume) resolution for NIM | PEPLO |
|---|
| PEH_IDLE_1 | IDLE may include a sensor on HV but not taking science data, values to be updated
* Macro: 100 | PEPHI |
|---|
| PEH_STBY_1 | Different STBY versions may include different sensors on, in Low voltage
* Macro: 100 | PEPHI |
|---|
| PEH_OFF_1 | PEP-Hi off
* Macro: 0 | PEPHI |
|---|
| PEH_GANYMEDE_IN_SITU_NOMINAL_1 | * Regular in-situ mode, ganymede phase
*CA of moon flybys later in the mission (higher power consumption)
*Good for high quality, extended survey
* Macro: 118
Sensors: JENI, JoEE | PEPHI |
|---|
| PEH_GANYMEDE_IN_SITU_BURST_1 | *Burst in-situ mode, ganymede phase
*CA of moon flybys
*Short duration events (e.g. boundary crossings)
* Macro: 122 | PEPHI |
|---|
| PEH_JUPITER_IN_SITU_IMAGING_LOW_1 | *Low power in-situ & ENA imaging mode (e.g. downlink, non-prime/low priority science sgments
* Macro: 142
Sensors: JENI, JoEE | PEPHI |
|---|
| PEH_JUPITER_IN_SITU_LOW_1 | *Low power in-situ mode
(e.g. downlink, non-prime/low priority science sgments)
* Macro: 110
Sensors: JENI, JoEE | PEPHI |
|---|
| PEH_JUPITER_IN_SITU_BURST_1 | *Burst in-situ mode, magnetosphere
*CA of moon flybys
*Short duration events (magnetopause/bow shock crossings, injection events, moon wakes/microsignatures)
* Macro: 121
Sensors: JENI, JoEE | PEPHI |
|---|
| PEH_JUPITER_IN_SITU_IMAGING_BURST_1 | *Regular magnetosphere in-situ
& ENA imaging monitoring mode
* Macro: 148b
Sensors ON: JENI, JoEE. | PEPHI |
|---|
| PEH_JUPITER_IN_SITU_NOMINAL_1 | *Regular magnetosphere in-situ
monitoring mode
*Can work on flybys
* Macro: 117
Sensors ON: JENI, JoEE | PEPHI |
|---|
| PEH_JUPITER_IN_SITU_IMAGING_NOMINAL_1 | *Low power in-situ & ENA imaging mode (e.g. downlink, non-prime/low priority science sgments
* Macro: 142
Sensors ON: JENI, JoEE | PEPHI |
|---|
| UVS_DECONTAMINATION | Not a true observation, but included so other instruments are aware that our heaters are on | UVS |
|---|
| UVS_CALIBRATION | Generic calibration observation - may include star stare, flip ridealong, or dark/radiation observations. Data rate is an estimated average. | UVS |
|---|
| UVS_IO_TORUS_SCAN | Map emissions from the Io torus. Slit aligned parallel with Jupiter's equator, scanned N-S across one ansa of the torus, then move in four steps to the other ansa, repeating the N-S motion each time | UVS |
|---|
| UVS_JUP_MONITORING_HP | As above, more of an auroral focus. 2-hour observations fit in between the AP monitoring observations | UVS |
|---|
| UVS_JUP_MONITORING_AP | Replaces previous monitoring stare. We perform a slow scan across the disk: assume 3 seconds per slit width, so 0.033 / s scan rate | UVS |
|---|
| SWI_2D_MAP_OTF_CCH_V1 | Similar to SWI 2D MAP PS, but using an on-the-fly recording sequence,
i.e. the OFF position per map row is only observed once. | SWI |
|---|
| SWI_2D_MAP_OTF_V1 | Similar to SWI 2D MAP PS, but using an on-the-fly recording sequence,
i.e. the OFF position per map row is only observed once. | SWI |
|---|
| SWI_NADIR_STARE_FS_V1 | Same as SWI NADIR STARE PS, except a frequency-switch calibration
mode is used instead of position-switch. It enables spending 100% of the integration time
on-source. If the purity of the spectral band is good enough, there is an option to pre-compute
ON-OFF for the CTS before downlink. | SWI |
|---|
| SWI_NADIR_STARE_PS_V1 | Investigation of the atmospheric composition (and temperature) of Jupiter
and the Galilean moons. This mode is nominally meant for deep integrations and requires numerous
repetitions (e.g. monitoring of the moons). Two CTS spectra are recorded for 60 seconds
over 10000 channels (16 bits coding). Position-switch calibration method. | SWI |
|---|
| SWI_TSYS_ACS_CCH_V1 | Spectral scan to measure the system temperature spectra of the 2 bands with
the ACS & CCH 1 & 2 by observing the hot load and cold sky. Integration time on ACS is 1
second. A single execution can cover up to 15 tunings. | SWI |
|---|
| UVS_SAT_LIMB_SCAN_HP | Similar to disc scan observations, but holding the pointing relative to the limb during flyby sequences. | UVS |
|---|
| UVS_SAT_LIMB_SCAN_AP | Similar to disc scan observations, but holding the pointing relative to the limb during flyby sequences. | UVS |
|---|
| UVS_SAT_LIMB_STARE_HP | Search for faint atmospheric emissions by building signal to noise through long integrations. | UVS |
|---|
| UVS_SAT_LIMB_STARE_AP | Search for faint atmospheric emissions by building signal to noise through long integrations. | UVS |
|---|
| UVS_SAT_DISK_SCAN_HP | Construct spectral image cubes of multiple atmospheric emission line features (up to 1024 selectable spectral bins with a minimum of 3 key emissions: H Lya, OI 130.4 nm, OI 135.6 nm), with repeated scans to investigate highly time-variable auroral dynamics. | UVS |
|---|
| UVS_SAT_DISK_SCAN_AP | Construct spectral image cubes of multiple atmospheric emission line features (up to 1024 selectable spectral bins with a minimum of 3 key emissions: H Lya, OI 130.4 nm, OI 135.6 nm), with repeated scans to investigate highly time-variable auroral dynamics. | UVS |
|---|
| UVS_NC_STARE | Characterize the Io/Europa neutral clouds in the immediate vicinity of the satellite. Center satellite in slit. Align the slit with the satellite orbital plane | UVS |
|---|
| UVS_IO_TORUS_STARE | Monitor emissions from the Io torus. Slit aligned parallel with Jupiter's equator. | UVS |
|---|
| UVS_GCO_HISTOGRAM_003 | Similar to observation 001 but with increased spectral resolution to achieve < 2 nm resolution between 100 and 200 nm as specified in SciRD | UVS |
|---|
| 3GM_BISTATIC_RADAR | Characterization of the surface by determination of roughness, dielectric constant of surface material and material density. The chosen antenna points towards surface, radio signal reflects from surface and received on ground.
USO unmuted.
The HAA shall be ON to calibrate the sloshing potentially excited by pointing the HGA toward a moon’s Surface. | 3GM |
|---|
| 3GM_OCCULTATION | The radio science experiment 3GM, with its dual-frequency radio links (X and Ka-band) referenced to an ultrastable oscillator (USO), is performed as JUICE spacecraft moves in and out of occultation. Occultations occur throughout the jovian tour, but their phasing is not always synchronized with the timing of dedicated Jupiter observations by the other orbiter experiments. USO unmuted, HAA in NOMINAL SCIENCE.
Note that 2 other options exist for torus occultations but are not (yet) defined in the database | 3GM |
|---|
| 3GM_GRAVITY_TOUR | KaT and HAA should be operating during gravity measurement
USO assumed to be ON during the full tour: this should be defined in the scenario set-up and not at 3GM observation approach.
HAA should be in STANDBY mode at least 48 hours before the gravity measurement.
The observation should start with 1 hour of HAA in CALIBRATION mode. KaT starts with 10min of warm-up. | 3GM |
|---|
| 3GM_GRAVITY_GCO500_200 | Gravity measurement during GCO500 and GCO200 will use the HGA during downlink sessions. If not possible, it will use the MGA. KaT and HAA should be operating during gravity measurement. USOis OFF during this phase (except in case of BSR opportunity). HAA should be in STANDBY mode at least 48 hours before the gravity measurement. The observation should start with 1 hour of HAA in CALIBRATION mode. KaT starts with 10min of warm-up. | 3GM |
|---|
| 3GM_GRAVITY_FLYBYS | Gravity measurement during flyby requires the use of the MGA.
KaT and HAA should be operating during gravity measurement
USO assumed to be ON during the full tour: this should be defined in the scenario set-up and not at 3GM observation approach.
HAA should be in STANDBY mode at least 48 hours before the gravity measurement.
The observation should start with 1 hour of HAA in CALIBRATION mode. KaT starts with 10min of warm-up. | 3GM |
|---|
| UVS_JUP_ROLL_SCAN | Point to nadir. Rotate about nadir so that we scan a circle (or a fraction of a circle - e.g. covering the auroral regions) over Jupiter's disk. Rotation rate ~0.1 degree per second | UVS |
|---|
| GAL_GAN_OFF_POINTING | specific observation for polar geometry with off-pointing w.r.t Nadir during GCO500.
Only to be executed TBD time. Similar profile than GAL_MONITORING_GAN but with off nadir pointing request | GALA |
|---|
| GAL_WARMUP_GAN | needed right before ANY science observation from GALA during Ganymede phase
Duration: 90min | GALA |
|---|
| JAN_SCI_INERTIAL | TBW | JANUS |
|---|
| JAN_SCI_LIMB | Children observations defined during scenarios
│ ├── JAN_SCI_LIMB_HAZES
│ ├── JAN_SCI_LIMB_HIGHPHASE
│ ├── JAN_SCI_LIMB_POLAR_SOUTH | JANUS |
|---|
| PEL_GANYMEDE_IN_SITU_LOW_7 | Mode with only NIM on (ion) from PEP-Lo. Required for avoiding switching on/off NIM once per day during downlinks. Good for long surveys of the ionosphere.
PEPLo Sensors ON: NIM ion on, only | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_LOW_6 | Mode with only NIM on (neutral) from PEP-Lo. Required for avoiding switching on/off NIM once per day during downlinks. Good for long surveys of the exosphere.
PEPLo Sensors ON: NIM neutral on, only | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_NOMINAL_3 | Regular in-situ mode, ganymede phase. CA of moon flybys later in the mission (higher power consumption). Good for high quality, extended survey in charged particles. NIM, JNA off.
PEPLo Sensors ON: JDC, JEI on, JNA & NIM off | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_NOMINAL_2 | Regular in-situ mode, ganymede phase. CA of moon flybys later in the mission (higher power consumption). Good for high quality, extended survey. All instruments on, NIM in ion mode (response of ionosphere to charged particles).
PEPLo Sensors ON: All sensors ON, NIM, JNA ion mode | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_NOMINAL_1 | Regular in-situ mode, ganymede phase. CA of moon flybys later in the mission (higher power consumption). Good for high quality, extended survey. All instruments on, NIM in neutral mode (response of exosphere to charged particles).
PEPLo Sensors ON: All sensors ON, NIM neutral mode, JNA ion mode | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_BURST_1 | Burst in-situ mode, Ganymede phase. CA of moon flybys later in the mission (higher power consumption) Short duration events (e.g. boundary crossings). All instruments on, NIM in neutral mode (response of ionosphere to charged particles). PEP Hi on, all in-situ
PEPLo Sensors ON: All sensors ON, NIM neutral mode, JNA ion mode | PEPLO |
|---|
| RIM_GANYMEDE_O1_1 | Ganymede Optional Acquisitions (O1) in low vertical resolution (LR) mode at high penetration depth until 15km considering on-board processing with presuming factor Np of 1. | RIME |
|---|
| RIM_GANYMEDE_O1_2 | Ganymede Optional Acquisitions (O1) in low vertical resolution (LR) mode at high penetration depth until 15km considering on-board processing with presuming factor Np of 2. | RIME |
|---|
| RIM_GANYMEDE_O1_4 | Ganymede Optional Acquisitions (O1) in low vertical resolution (LR) mode at high penetration depth until 15km processing with presuming factor Np of 4. | RIME |
|---|
| RIM_GANYMEDE_N4 | Passive Radar Acquisitions on Jovian side of Ganymede. | RIME |
|---|
| RIM_GANYMEDE_N3_1 | Ganymede Nominal Acquisitions (N3) in high vertical resolution (HR) mode until 4km depth in the anti-Jovian side of Ganymede in order to complete the SRM on high-interest targets considering on-board processing with presuming factor Np of 1. | RIME |
|---|
| RIM_GANYMEDE_N3_2 | Ganymede Nominal Acquisitions (N3) in high vertical resolution (HR) mode until 4km depth in the anti-Jovian side of Ganymede in order to complete the SRM on high-interest targets considering on-board processing with presuming factor Np of 2. | RIME |
|---|
| RIM_GANYMEDE_N3_4 | Ganymede Nominal Acquisitions (N3) in high vertical resolution (HR) mode until 4km depth in the anti-Jovian side of Ganymede in order to complete the SRM on high-interest targets considering on-board processing with presuming factor Np of 4. | RIME |
|---|
| RIM_GANYMEDE_N2_1 | Ganymede Nominal Acquisitions (N2): in low vertical resolution (LR) mode until 9km depth in the Jovian side of Ganymede considering on-board processing with presuming factor Np of 1. | RIME |
|---|
| RIM_GANYMEDE_N2_2 | Ganymede Nominal Acquisitions (N2): in low vertical resolution (LR) mode until 9km depth in the Jovian side of Ganymede considering on-board processing with presuming factor Np of 2. | RIME |
|---|
| RIM_GANYMEDE_N2_4 | Ganymede Nominal Acquisitions (N2): in low vertical resolution (LR) mode until 9km depth in the Jovian side of Ganymede considering on-board processing with presuming factor Np of 4. | RIME |
|---|
| RIM_GANYMEDE_N1_1 | Ganymede Nominal Acquisitions (N1) in low vertical resolution (LR) mode until 9km depth in the anti-Jovian side of Ganymede considering on-board processing with presuming factor Np of 1. | RIME |
|---|
| RIM_GANYMEDE_N1_2 | Ganymede Nominal Acquisitions (N1) in low vertical resolution (LR) mode until 9km depth in the anti-Jovian side of Ganymede considering on-board processing with presuming factor Np of 2. | RIME |
|---|
| RIM_GANYMEDE_N1_4 | Ganymede Nominal Acquisitions (N1) in low vertical resolution (LR) mode until 9km depth in the anti-Jovian side of Ganymede considering on-board processing with presuming factor Np of 4. | RIME |
|---|
| RIM_GANYMEDE_FLYBY | RIME flyby observations or observations without on-board processing. | RIME |
|---|
| NAVCAM_DVOL_BLOCK | | JUICE |
|---|
| MAG_DL_FOB_LIGHT_ONLY | This observation is introduced to characterise JMAG operations during downlink times where power resources from the SC may be more limited, and where SC attitude is driven by operational constraints In this particular observation FOB fluxgate is powered on with FSC as light-only. | JMAG |
|---|
| MAG_DL_LIGHT_ONLY | This observation is introduced to characterise JMAG operations during downlink times where power resources from the SC may be more limited, and where SC attitude is driven by operational constraints.
In this particular observation FIB & FOB fluxgates powered on with FSC as light-only. | JMAG |
|---|
| PEL_GANYMEDE_IN_SITU_LOW_2 | Same as PEP_GANYMEDE_IN_SITU_NOMINAL_1 but with low performance in JDC, JEI to limit power (JE 4 sectors, JDC low power). NIM neutral, JNA on. Low power mode for Ganymede, good for long duration surveys with multiple instruments.
PEPLo Sensors ON: JEI: 4 sectors, JDC: LP, NIM: Neutral mode | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_LOW_5 | Same as PEP_GANYMEDE_IN_SITU_LOW_1 but with lowest performance in JDC, JEI for max power savings while PEP-Lo is no (JEI 4 sectors, JDC low power). NIM, JNA off. Low power mode for Ganymede, good for long duration surveys.
PEPLo Sensors ON: JDC_LP, JEI 4 sectors, JNA & NIM off | PEPLO |
|---|
| PEL_JUPITER_IN_SITU_LOW_1 | Low power in-situ mode (e.g. downlink, non-prime/low priority science sgments)
PEPLo Sensors ON: JDC_LP, JEI (8 sectors) | PEPLO |
|---|
| PEL_JUPITER_IN_SITU_BURST_1 | Burst in-situ mode for magnetosphere, CA of moon flybys (if NIM offl), Short duration events (magnetopause/bow shock crossings, injection events, moon wakes/microsignatures)
PEPLo Sensors ON: JDC, JEI | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_LOW_3 | Same as PEP_GANYMEDE_IN_SITU_NOMINAL_1 but with low performance in JDC, JEI to limit power (JEI 4 sectors, JDC low power). NIM ion, JNA on. Low power mode for Ganymede, good for long duration surveys with multiple instruments.
PEPLo Sensors ON: JEI: 4 sectors, JDC: LP, NIM: Ion mode | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_LOW_4 | Same as PEP_GANYMEDE_IN_SITU_NOMINAL_1 but with low performance in JDC, JEI to limit power (JEI 4 sectors, JDC low power). NIM ion, JNA on. Low power mode for Ganymede, good for long duration surveys with multiple instruments.
PEPLo Sensors ON: JEI: 4 sectors, JDC: LP, NIM: Ion mode | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_BURST_2 | Burst in-situ mode, Ganymede phase. CA of moon flybys later in the mission (higher power consumption) Short duration events (e.g. boundary crossings). All instruments on, NIM in neutral mode (response of ionosphere to charged particles). PEP Hi on, all in-situ
PEPLo Sensors ON: All sensors ON, NIM, JNA ion mode | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_LOW_1 | Same as PEP_GANYMEDE_IN_SITU_NOMINAL_3 but with low performance in JDC, JEI to limit power (JEI 8 sectors, JDC low power). NIM, JNA off. Low power mode for Ganymede, good for long duration surveys
PEPLo Sensors ON: JDC_LP, JEI (8 sectors) | PEPLO |
|---|
| MAG_CONTINOP_FIB_FOB_LIGHT_ONLY | JMAG mode (FIB FOB Light Only), this mode ensures that while FIB and FOB are collecting science the Scalar sensor also has power to its laser but is not collecting science data. This helps to protect the fibres from radiation damage, necessary for the Europa phase due to its radiation environment. | JMAG |
|---|
| SWI_SCIENCE | Place holder:
one of the ASW mode, where the science script will be run ( i.e. from SWI_TSYS_CTS down to SWI_MOON_NADIR_STARE_FS) during the mission | SWI |
|---|
| SWI_SPECTRAL_SCAN_CTS_FS_V1 | Same as SWI SPECTRAL SCAN CTS PS, except a frequency-switch calibration
mode is used instead of position-switch. It enables spending 100% of the integration
time on-source. If the purity of the spectral band is good enough, there is an option to precompute
ON-OFF for the CTS before downlink. A single execution can cover up to 9 tunings. | SWI |
|---|
| SWI_SPECTRAL_SCAN_CTS_PS_V1 | Investigation of the atmospheric composition of Jupiter and the Galilean
moons. The whole frequency range available to SWI is scanned. This mode is nominally meant for deep integrations and requires numerous repetitions (e.g. monitoring of the moons). Two
CTS spectra are recorded for 60 seconds over 10000 channels (16bit coding). Position-switch
calibration method. A single execution can cover up to 13 tunings.
Pointing Type: S/C: nadir or limb. Instrument: nadir or limb, using the SWI mechanism if S/C points
nadir and to reach the moons | SWI |
|---|
| SWI_SPECTRAL_SCAN_ACS_FS_V1 | Same as SWI SPECTRAL SCAN ACS PS, except a frequency-switch calibration
mode is used instead of position-switch. It enables spending 100% of the integration
time on-source. The ACS does not allow to pre-compute ON/OFF before downlink. A single
execution can cover up to 11 tunings. | SWI |
|---|
| SWI_SPECTRAL_SCAN_ACS_PS_V1 | Investigation of the atmospheric composition of Jupiter and the Galilean
moons. The whole frequency range available to SWI is scanned. This mode is nominally meant
for deep integrations and requires numerous repetitions (e.g. monitoring of the moons). Two
ACS spectra are recorded for 60 seconds over 1024 channels. Position-switch calibration method.
A single execution can cover up to 16 tunings. | SWI |
|---|
| PEL_JUPITER_IN_SITU_IMAGING_NOMINAL_3 | Legacy description from PEP_FLYBY_CLOSEST_APPROACH:
Local moon-magnetosphere interaction observation: plasma moments, energetic particle spectra and pitch angle distributions (high time resolution for short term variations)
Europa imaging (JNA). Dense exosphere (NIM)
Sensors on: all
Corotation in JEI or JDC FoV
Full pitch angle coverage (JDC, JEI, JoEE, JENI)
Moon in JNA FoV
Angle of NIM_NEUION_S0 from JUICE_EUROPA_RAM or JUICE_GANYMEDE_RAM or JUICE_CALLISTO_RAM velocity less than 5 deg at CA
Solar panel rotation angle (SADM) SADM > 74° or
SADM < -74°
Moon in JNA FoV | PEPLO |
|---|
| PEL_JUPITER_IN_SITU_IMAGING_NOMINAL_2 | Configuration just before moon CA (flyby)
Legacy description (when it was called PEP_FLYBY_APPROACH):
Moon environment monitoring: plasma moments, energetic particle spectra and pitch angle distributions (low time resolution). Moon imaging (JNA) & Europa torus (JNA imaging + in-situ) if near Europa. High altitude exosphere (NIM)
Sensors on: all
Corotation in JEI or JDC FoV
Full pitch angle coverage (JDC, JEI, JoEE, JENI ions)
Moon in JNA FoV
Angle of NIM_THERMAL_1 or THERMAL_2 from
JUICE_EUROPA_RAM or JUICE_GANYMEDE_RAM or JUICE_CALLISTO_RAM velocity less than 60 deg | PEPLO |
|---|
| PEL_JUPITER_IN_SITU_IMAGING_LOW_5 | Far approach from moon (flyby), NIM thermal, medium resolution
Legacy description from PEP_FLYBY_FAR_APPROACH_MEDIUM_RATE
Moon environment monitoring: plasma moments, energetic particle spectra and pitch angle distributions (low time resolution). Europa torus (JNA imaging + in-situ) if near Europa
Sensors on: all
Corotation in JEI or JDC FoV
Full pitch angle coverage (JDC, JEI, JoEE, JENI ions)
Moon in JNA FoV
Angle of NIM_THERMAL_1 or THERMAL_2 from
JUICE_EUROPA_RAM or JUICE_GANYMEDE_RAM or JUICE_CALLISTO_RAM velocity less than 60 deg | PEPLO |
|---|
| PEL_JUPITER_IN_SITU_IMAGING_LOW_4 | Far approach from moon (flyby), NIM thermal, low resolution
Legacy description from PEP_FLYBY_FAR_APPROACH_LOW_RATE
Moon environment monitoring: plasma moments, energetic particle spectra and pitch angle distributions (low time resolution). Europa torus (JNA imaging + in-situ) if near Europa
Sensors on: all
Corotation in JEI or JDC FoV
Full pitch angle coverage (JDC, JEI, JoEE, JENI ions) | PEPLO |
|---|
| PEL_JUPITER_IN_SITU_IMAGING_LOW_3 | Far approach from moon (flyby), NIM background measurements
Legacy description from PEP_FLYBY_FAR_APPROACH_NIM_BACKGROUND:
NIM background measurements part of switch on procedure.
Moon environment monitoring: plasma moments, energetic particle spectra and pitch angle distributions (low time resolution). Europa torus (JNA imaging + in-situ) if near Europa
Sensors on: all
Corotation in JEI or JDC FoV
Full pitch angle coverage (JDC, JEI, JoEE, JENI ions) | PEPLO |
|---|
| RIM_EUROPA_FLYBY | RIME flyby observations or observations without on-board processing | RIME |
|---|
| UVS_IRR_SAT | Obtain reflectance spectra of irregular satellites | UVS |
|---|
| UVS_IO_SCAN | Similar to UVS_DISK_SCAN, but including extra emission lines e.g. from S and Cl. Also requires different spatial binning since Io is more distant | UVS |
|---|
| UVS_SAT_TRANSIT | Measure absorption of Jupiter airglow by satellite atmospheres as they transit Jupiter's disk, to constrain satellite atmospheric composition and variability.
Pointing: nadir (Point slit N-S on Jupiter's disk and wait for moon to transit) | UVS |
|---|
| UVS_EUR_SCAN_HIGH_RES_OBSOLETE | Similar to UVS_DISK_SCAN but higher resolution.
pointing: start at -1.5 satellite radii from the satellite centre, scan in the direction perpendicular to the slit across the disk, ending at +1.5 satellite radii from the centre | UVS |
|---|
| UVS_SAT_SURF_HP | As UVS_SAT_SURF_AP but using the high resolution port for improved spatial resolution in key surface regions | UVS |
|---|
| UVS_SAT_SURF_AP | Pushbroom observations near flyby closest approach to investigate surface composition | UVS |
|---|
| MAJ_STANDBY | After switch-on of MAJIS, the Boot SW automatically starts, and performs the primary boot from the PROM (Init fugitive BSW mode).
After processor modules initialization, the Boot software goes to STANDBY mode. By default, the ASW Image0 (stored in MRAM0 = ASM0) is autonomously loaded after a timeout of 30 seconds. MAJIS then enters into ASW init Mode and then into SAFE mode.
In STANDBY Mode, all channels are off, and only DPU HK SID1 are received.
MAJIS needs to be maintained in STANDBY mode using the TC(17,1) in the following cases :
- upload (using service 6) of new ASW images (or CUSW, or firmware) into MRAM: FCP-MAJ-070 describes the maintenance process.
- upload a new BROWSE Table FCP-MAJ-060 into MRAM
- select ASW Image1 and then start ASW Image 1 instead of teh default ASW Image0. FCP-MAJ-062
- any other update of MRAM using service 6 | MAJIS |
|---|
| MAJ_SERVICE | MAJIS in service MODE (1 or 2 channels with FPE/FPA off + AUX w/o loads)
SERVICE Mode as soon as one or two channels are switched ON (PE and AUX)
From SERVICE, it is possible to return to SAFE mode or to change the status of MAJIS to DIAG2, DIAG3 or SCIENCE
Duration: less than 10min | MAJIS |
|---|
| MAJ_SAT_LIMB_TRACK | Continuous stare observation of a satellite limb during flyby using inertial pointing from satellite, dayside or nightside. Additional offsets within limb by means of internal pointing mirror. Scanning with MAJIS internal mirror. (--> ‘track limb’).
Pointing: S/C limb tracking (‘track limb’)
satellite otientation: SLIT tangent to the limb (slit not aligned with S/C motion)
Duration: 60min | MAJIS |
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| MAJ_SAT_LIMB_SCAN | Flyby observations of the satellite dayside or nightside limbs with vertical (N-S) slews across track, during yaw-steering phase. Satellite offsets to limb around Y-axis (E-W) before each observation, then satellite offsets around X axis (N-S) between each slit acquisition or continuous slew pointing.
Pointing: S/C slew scan centred a limb ( ‘Limb slew scan mode’).
Satelliteo orientation: Slit tangent to the limb
Duration: 60min | MAJIS |
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| MAJ_SAT_DISK_SLEW | Flyby observations of the satellite surface with vertical (N-S) slews across track, during yaw-steering phase. One or two slews (pole to pole) necessary to complete dayside coverage. Satellite offset around Y-axis (E-W) before each observation, then satellite offsets around X axis (N-S) between each slit acquisition.
Pointing: NADIR Pointing, YS, S/C scan (slew) with offset around Y (‘mosaic mode’ tbc). MAJIS slit perpendicular to the ground-track.
Satellite orientation: MAJIS slit perpendicular to the ground-track
Duration: 30 min | MAJIS |
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| MAJ_SAT_DISK_SCAN | Observation of a distant satellite dayside or nightside surface. Satellite offset required for pointing then disk coverage is achieved using the internal pointing mirror scanning in the Y (N-S) direction.
Pointing: NADIR-P with possible offset around Y, YS, MAJIS scan (‘Nadir scan’).
Satellite orientation: MAJIS slit perpendicular to the ground-track
Duration: 30min | MAJIS |
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| MAJ_SAFE | Initiated after ASW loading
All channels are off and no PE HK are generated. Only ME HK are generated (only DPU ON)
From SAFE it is possible 1) to switch OFF MAJIS, 2) to change the status of MAJIS to DIAG1 or SERVICE mode
Duration: less than 5min | MAJIS |
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| MAJ_Ring_Occultation | Observation of a star occulted by the rings
Scan windowing of 9 lines centered on the star (1 scan step = 1/3 MAJIS IFOV) possible
Pointing: Inertial. For each occultation, transit of TBD min
Satellite orientation: Inertial pointing of the S/C towards the position of the star to maintain MAJIS slit fixed on it. These occultation observations need to be consolidated in the future (star atlas, signal, Tint, S/C inertial capabilities). Scan mirror can be used to mitigate APE drift | MAJIS |
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